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J/A+A/614/A135        Spectra of 78 PN central stars          (Weidmann+, 2018)

Towards an improvement in the spectral description of central stars of planetary nebulae. Weidmann W., Gamen R., Mast D., Farina C., Gimeno G., Schmidt E.O., Ashley R.P., Peralta de Arriba L., Sowicka P., Ordonez-Etxeberria I. <Astron. Astrophys. 614, A135 (2018)> =2018A&A...614A.135W (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Planetary nebulae ; Stars, population II Keywords: planetary nebulae: general - stars: Population II - stars: early-type - surveys Abstract: There are more than 3000 known Galactic planetary nebulae (PNe), but only 492 central stars of Galactic planetary nebulae (CSPN) have known spectral types. It is vital to increase this number in order to have reliable statistics, which will lead to an increase of our understanding of these amazing objects. We aim to contribute to the knowledge of central stars of planetary nebulae and stellar evolution. This observational study is based on Gemini Multi-Object Spectrographs (GMOS) and with the Intermediate Dispersion Spectrograph (IDS) at the Isaac Newton Telescope (INT) spectra of 78 CSPN. The objects were selected because they did not have any previous classification, or the present classification is ambiguous. These new high quality spectra allowed us to identify the key stellar lines for determining spectral classification in the Morgan-Keenan (MK) system. We have acquired optical spectra of a large sample of CSPN. From the observed targets, 50 are classified here for the first time while for 28 the existing classifications have been improved. In seven objects we have identified a P-Cygni profile at the HeI lines. Six of these CSPN are late O-type. The vast majority of the stars in the sample exhibit an absorption-type spectrum, and in one case we have found wide emission lines typical of [WR] stars. We give a complementary, and preliminary, classification criterion to obtain the sub-type of the O(H)-type CSPN. Finally, we give a more realistic value of the proportion of CSPN that are rich or poor in hydrogen. Description: Spectral classification of 78 central stars of Galactic planetary nebulae. The spectra were obtained with Gemini Multi-Object Spectrographs (GMOS) and with the Intermediate Dispersion Spectrograph (IDS) at the Isaac Newton Telescope (INT). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea3.dat 112 78 Spectral types from our observations fits/* 0 81 Individual fits spectrum files
See also: V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992) J/A+A/526/A6 : Central stars of planetary nebulae (Weidmann+, 2011) J/A+A/531/A172 : Central stars of planetary nebulae. II. (Weidmann+, 2011) Byte-by-byte Description of file: tablea3.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq Sequential number 4- 17 A14 --- Name Main designation 19- 28 A10 --- PNG PNG name (based on galactic position) 30- 46 A17 --- SpType Spectral type of central star (1) 48 A1 --- Tel [GI] Telescope (G: GEMINI/GMOS, I: INT/IDS) 50- 51 A2 --- HeII4542 [AE-? ] HeII at 4542Å detection flag (2) 53- 56 A4 --- HeII4686 [AE-?+ N/D] HeII at 4686Å detection flag (2) 58- 60 A3 --- HeII5412 [AE-? N/D] HeII at 5412Å detection flag (2) 62- 63 A2 --- HeI4471 [AE-? ] HeI at 4471Å detection flag (2) 65- 66 A2 --- Hb4861 [AE-? ] Hβ detection flag (2) 68- 69 A2 --- NV4603 [AE-? ] NV at 4603-4619Å detection flag (2) 71- 74 A4 --- CIV5806 [AE-?+ N/D] CIV at 5801-5812Å detection flag (2) 76 A1 --- NS [y/n] Indicates whether or not it was possible to subtract the nebular component. 78- 93 A16 --- FileName Name of the spectrum file in subdirectory fits 94 A1 --- --- [,] 96-112 A17 --- FileName2 Name of second spectrum file in subdirectory fits
Note (1): Spectral types as follows: O(H) = Balmer and HeII absorption lines detected H-rich = Balmer lines detected but neither HeI or HeII O = Only HeII absorptions lines detected cont. = A high S/N spectrum in which no stellar features and HeII emission lines were detected Emission line = Spectrum where no absorption lines are present but the observed emission lines have a stellar origin Note (2): Detection flags as follows: A = absorption E = emission - = undetected ion N/D = data available
Acknowledgements: Walter Alfredo Weidmann, walter(at)
(End) Walter A. Weidmann [OAC, Argentina], Patricia Vannier [CDS] 05-Feb-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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